BLAST: CORRELATIONS IN THE COSMIC FAR-INFRARED BACKGROUND AT 250, 350, AND 500 μm REVEAL CLUSTERING OF STAR-FORMING GALAXIES
BLAST: CORRELATIONS IN THE COSMIC FAR-INFRARED BACKGROUND AT 250, 350, AND 500 μm REVEAL CLUSTERING OF STAR-FORMING GALAXIES
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爆炸：250、350 和 500 μm 宇宙远红外背景的相关性揭示了恒星形成星系团
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发表时间：
2009
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通讯作者：
D. Wiebe
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作者：
M. Viero;P. Ade;J. Bock;E. Chapin;M. Devlin;M. Griffin;J. Gundersen;M. Halpern;P. Hargrave;D. Hughes;J. Klein;C. MacTavish;G. Marsden;P. Martin;P. Mauskopf;L. Moncelsi;M. Negrello;C. Netterfield;L. Olmi;E. Pascale;G. Patanchon;M. Rex;D. Scott;C. Semisch;N. Thomas;M. Truch;C. Tucker;G. Tucker;D. Wiebe
我们探测到宇宙远红外背景中的相关性，这是由于在250、350和500 μm处用星载大孔径亚毫米望远镜进行的观测中恒星形成星系的聚集。我们执行折叠和其他测试来确认信号的真实性。在5′ ~ 25 ′尺度范围内，测量的相关系数符合幂律，ΔI/I = 15.1% ± 1.7%。我们采用了一个特定的亚毫米波源模型，其中对聚类的贡献来自红移范围为1.3 <$z <$2.2，1.5 <$z <$2.7和1.7 <$z <$3.2的源，分别在250，350和500 μm。利用这些分布，我们对功率谱P（kθ）的测量分别对应于线性偏置参数B = 3.8 ± 0.6、3.9 ± 0.6和4.4 ± 0.7。我们进一步解释的晕模型的结果，并发现，在较小的尺度，最简单的晕模型无法拟合我们的结果。改善拟合的一种方法是增加暗物质晕在模型中被人为截断的半径，这相当于让一些恒星形成星系位于z = 1的星系群和星系团的外围。在这个模型的背景下，我们发现一个星系所需的最小晕质量是log（Mmin/M返）= 11.5+0.4−0.1，我们推导出有效偏差beff = 2.2 ± 0.2，2.4 ± 0.2和2.6 ± 0.2，有效质量为12.8 ± 0.2和12.7 ± 0.2，在250，350和500 μm，分别对应于r 0 = 4.9、5.0和5.0的空间相关长度。最后，我们讨论了集群测量策略与赫歇尔和普朗克的影响。
We detect correlations in the cosmic far-infrared background due to the clustering of star-forming galaxies in observations made with the Balloon-borne Large Aperture Submillimeter Telescope, at 250, 350, and 500 μm. We perform jackknife and other tests to confirm the reality of the signal. The measured correlations are well fitted by a power law over scales of 5′–25′, with ΔI/I = 15.1% ± 1.7%. We adopt a specific model for submillimeter sources in which the contribution to clustering comes from sources in the redshift ranges 1.3 ⩽ z ⩽ 2.2, 1.5 ⩽ z ⩽ 2.7, and 1.7 ⩽ z ⩽ 3.2, at 250, 350, and 500 μm, respectively. With these distributions, our measurement of the power spectrum, P(kθ), corresponds to linear bias parameters, b = 3.8 ± 0.6, 3.9 ± 0.6, and 4.4 ± 0.7, respectively. We further interpret the results in terms of the halo model, and find that at the smaller scales, the simplest halo model fails to fit our results. One way to improve the fit is to increase the radius at which dark matter halos are artificially truncated in the model, which is equivalent to having some star-forming galaxies at z ⩾ 1 located in the outskirts of groups and clusters. In the context of this model, we find a minimum halo mass required to host a galaxy is log(Mmin/M☉) = 11.5+0.4−0.1, and we derive effective biases beff = 2.2 ± 0.2, 2.4 ± 0.2, and 2.6 ± 0.2, and effective masses , 12.8 ± 0.2, and 12.7 ± 0.2, at 250, 350 and 500 μm, corresponding to spatial correlation lengths of r0 = 4.9, 5.0, and , respectively. Finally, we discuss implications for clustering measurement strategies with Herschel and Planck.